GRB 100119A

V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
S. Campana (INAF-OAB), P.A. Curran (MSSL-UCL),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
K. L. Page (U Leicester), J. L. Racusin (NASA/GSFC),
T. Sakamoto (NASA/UMBC), M. H. Siegel (PSU), M. C. Stroh (PSU),
T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the
Swift Team:

At 18:25:25 UT, the Swift Burst Alert Telescope (BAT) triggered and  
located GRB 100119A (trigger=383063).  Swift did not slew because
of a Sun observing constraint. 
The BAT on-board calculated location is
RA, Dec 299.327, -53.160 which is
   RA(J2000)  =  19h 57m 18s
   Dec(J2000) = -53d 09' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The BAT light curve shows multiple overlapping
peaks with a duration of about 25 sec.  The peak count rate
was ~6000 counts/sec (15-350 keV), at T+5 sec. 

Due to an observing constraint, Swift cannot slew to the BAT position. 
There will thus be no XRT or UVOT data for this trigger. No observations 
with XRT or UVOT will be possible for approximately the next 26 days. 

Burst Advocate for this burst is V. Mangano (vanessa AT ifc.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
V. Mangano (INAF-IASFPA), C. B. Markwardt (GSFC/UMD), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 100119A (trigger #383063)
(Mangano, et al., GCN Circ. 10348
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 ).  The BAT ground-calculated position is
RA, Dec = 299.308, -53.149 deg which is 
   RA(J2000)  =  19h 57m 14.0s 
   Dec(J2000) = -53d 08' 56.7" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 7%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-30 sec, peaking at ~T+3 sec, and ending at ~T+30 sec.
T90 (15-350 keV) is 23.8 +- 4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-15.8 to T+15.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.01 +- 0.06.  The fluence in the 15-150 keV band is 1.4 +- 0.0 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+2.12 sec in the 15-150 keV band
is 7.7 +- 1.0 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/383063/BA/

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long GRB 100119A (Swift-BAT trigger=383063:
Mangano et al., GCN 10348
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 ) triggered Konus-Wind
at T0=66306.167s UT (18:25:06.167)

The burst light curve shows a complex structure
with a total duration of ~45 s.
The emission is seen up to several MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB100119_T66306/

As observed by Konus-Wind the burst
had a fluence of 6.1(+/-0.3)x10-5 erg/cm2,
and a 256-ms peak flux measured from T0+18.176s
of 4.3(+/-0.3)x10-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+37.376 s) is well be fitted
in the 20 keV - 10 MeV range by a power law
with GRB (Band) model, for which:
the low-energy photon index alpha = -0.73 (-0.08,+0.09),
the high energy photon index beta = -2.8(-1.9, +0.4),
the peak energy Ep = 377(-35, +35)keV (chi2 = 66/97 dof).

The spectrum of the most intense part of the burst
(measured from T0+15.360 to T0+21.504 s) is well fitted
in the 20 keV - 10 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.52(+/-0.11),
and Ep = 387(-32, +37) keV (chi2 = 97/96 dof).

All the quoted results are preliminary.
All the quoted errors are at the 90% confidence level.

=========================================================================

N. Vasquez (Tokyo Tech.), K. Yamaoka (Aoyama Gakuin U.),
T. Uehara, Y.Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.)
S. Sugita (Nagoya U), M. Tashiro, Y. Terada, A. Endo,
K. Onda, T. Sugasahara, W. Iwakiri (Saitama U.),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji,
E. Sonoda, K. Kono, H. Hayashi, K. Noda, Y. Nishioka, M. Yamauchi
(Univ. of Miyazaki), Y. Urata, H. M. Lin (NCU),
T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong
(Nihon U.), on behalf of the Suzaku WAM team, report:

The long GRB 100119A (Swift BAT trigger #383063; Mangano et al. GCN 10348
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 )
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 18:25:09.630 UT (=T0).

The observed light curve shows a complicated structure, with
overlapping pulses. The duration (T90) was about 24 seconds.
The fluence in 100 - 1000 keV band is 4.55(-0.21, +0.17) x 10^-6 erg/cm2
with a 1-s peak flux measured from T0+18.5 sec of 6.94 (-0.63, +0.32)
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0-3.5 s to T0+37.5 s is well fitted by a cut off power-law model:
 dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
 alpha      1.17 (-0.27, +0.26), and
 Epeak      510 (-45, +54) keV (chi^2/d.o.f. = 26.7/24).

Due to the brightness of this burst, a 3% systematic error
was added for low energy channels.
All the quoted errors are at 90% confidence level.

The light curves of this event are available at the following URL:
 http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html

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